On the high coherence of kHz quasi-periodic oscillations

Abstract

We have carried out a systematic study of the properties of the kHz quasi-periodic oscillations (QPOs) observed in the X-ray emission of the neutron star low-mass X-ray binary 4U 160852, using archival data obtained with the Rossi X-ray Timing Explorer. We have investigated the quality factor, Q, of the oscillations (defined as the ratio, /, of the frequency of the QPO peak to its full width at half-maximum ). In order to minimize the effect of long-term frequency drifts, power spectra were computed over the shortest times permitted by the data statistics. We show that the high Q of 200 reported previously for the lower-frequency kHz QPO is by no means exceptional, as we observe a mean Q value in excess of 150 in 14 out of the 21 observations analysed and Q can remain above 200 for thousands of seconds. The frequency of the QPO varies over the wide range 560890 Hz and we find a systematic trend for the coherence time of the QPO, estimated as =Q/() = 1/(), to increase with , up to a maximum level at 800 Hz, beyond which it appears to decrease, at frequencies where the QPO weakens. There is a more complex relationship between and the QPO rms amplitude, in which positive and negative correlations can be found. A higher-frequency QPO, revealed by correcting for the frequency drift of the 560890 Hz one, has a much lower Q (10) which does not follow the same pattern. We discuss these results in the framework of competing QPO models and we show that those involving clumps orbiting within or above the accretion disc are ruled out

Evolution of the 0.01–25 Hz power spectral components in Cygnus X-1

“…While this property makes the models good candidates in explaining the high coherence seen in higher frequency QPO's (Barret et al 2004), it also makes it difficult to explain the large (over one order of magnitude) shifts in peak frequency observed in our study. In addition, the features we model with Lorentzians have low coherence.…”

High frequency QPOs, nonlinear oscillations in strong gravity

“…It had been known that clumps in the differentially rotating accretion disk would be sheared out into nearly axisymmetric structures within a few orbits (Bath, Evans and Papaloizou 1974)-i.e., a clump is short livedand it has simply been overlooked that the kHz QPOs were reported to be very narrow features already in the discovery papers. Today we know that the high quality factor, Q ∼ 200 of the lower kHz QPOs in neutron-stars excludes all clumpbased models, as well as those involving longer-lived vortices drifting radially inwards with the mean accretion flow (Barret et al 2005). Thus, the question of relative merits of the "beat frequency model" and the "relativistic precession model" is a moot point.…”

Quasi-periodic oscillations under wavelet microscope: the application of Matching Pursuit algorithm

“…While this is useful in tracing the evolution of the QPO (e.g. Wilms et al 2001;Barret et al 2005), it introduces "instrumental" frequency broadening from the windowing of the data which prevents us following the detailed behaviour of the QPO on the required timescales.…”